Mass Loss and Non-Radial Pulsations in Be Stars
The interpretation of infra-red observations of Be stars made with IRAS is discussed. This shows that a slow stellar wind is leaving the star forming an equatorial disc. The mass loss rate is 50 to 100 times greater than that deduced from the ultraviolet observations, which show a fast rapidly accelerating wind coming presumably from the star outside the equatorial region. The large mass loss and slow velocities imply a mechanism for the stellar wind in the equatorial regions which is different from the radiatively driven wind.
The observations of non-radial pulsations in Be stars which have their maximum amplitude confined to the equatorial regions suggest a possible origin of the mass loss forming the disc. A theory of mass loss driven by sound waves is given. It is assumed that the sound wave are generated by the non-radial pulsations. This mechanism does give a slow stellar wind, but further work is necessary to find out whether the theory can explain the Be star observations.
KeywordsMass Loss Neutron Star Sound Wave Mass Loss Rate Stellar Wind
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